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UNIVERSITY of CALIFORNIA RIVERSIDE Black Hole Feedback UNIVERSITY OF CALIFORNIA RIVERSIDE Black Hole Feedback in Dwarf Galaxy Evolution A Dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Physics by Christina Manzano King September 2020 Dissertation Committee: Prof. Gabriela Canalizo, Chairperson Prof. Frederick Hamann Prof. Brian Siana Copyright by Christina Manzano King 2020 The Dissertation of Christina Manzano King is approved: Committee Chairperson University of California, Riverside Acknowledgments I would like to express my sincere gratitude to my advisor Prof. Canalizo for her continued patience and hard work mentoring me. I would also like to thank the rest of my thesis committee for their insightful comments, my group for their continued help throughout this project, and my friends in POWUR who held me up along the way. To those defending the sacred: Kū Kia‘i Mauna! iv I dedicate my work to Jose Lucero Manzano and Valentina Tuazon Manzano, who dreamt that their granddaughter would earn the family’s first doctorate degree, and to Ruena Manzano, who supports me in all I do. v ABSTRACT OF THE DISSERTATION Black Hole Feedback in Dwarf Galaxy Evolution by Christina Manzano King Doctor of Philosophy, Graduate Program in Physics University of California, Riverside, September 2020 Prof. Gabriela Canalizo, Chairperson In a scenario where all galaxies form and evolve with supermassive black holes in their centers, it is thought that these central black holes play a vital role in limiting the growth of massive galaxies. In order to extend our understanding of black hole influence on galaxy evolution into the low mass regime, we collected spatially resolved spectra of 10 50 nearby (z < 0:05) dwarf (M? < 10 M⊙) galaxies, selected from SDSS DR7 and DR 8 followed-up with Keck/LRIS spectroscopy. We study the potential effects of active galactic nuclei (AGN) on galaxy-wide gas kinematics and integrated stellar properties by comparing measurements obtained from 29 galaxies containing AGN, and 21 control galaxies with no optical or infrared signs of AGN. We present the first direct measurements of AGN-driven gas outflows in the low mass regime. We also find a strong association betweenAGN and disturbed ionized gas kinematics and signs of star formation suppression. Our results provide evidence that AGN can have significant influence on large scale gas motions in their host galaxies and their global stellar populations. AGN feedback appears to be an vi important, and perhaps dominant, mechanism that regulates dwarf galaxy evolution, and should be included in realistic galaxy formation models in the low-mass regime. vii Contents List of Figures 3 List of Tables 16 1 Introduction 1 Introduction . 1 1.1 Small Scale Problems . 2 1.2 An Overview of Baryonic Feedback . 5 1.2.1 Stellar feedback . 5 1.2.2 AGN feedback . 5 1.3 This Work . 7 2 Outflows 8 2.1 Introduction . 9 2.2 Data . 12 2.2.1 Sample Selection . 12 2.2.2 Observations and Data Reduction . 14 2.3 Analysis . 17 2.3.1 Fitting the Stellar Continuum . 18 2.3.2 Fitting Emission Lines . 19 2.3.3 Detecting Outflows . 21 2.3.4 Outflow Velocity . 22 2.3.5 Decomposed Flux Ratios . 23 2.4 Results . 24 2.4.1 Classifying Outflows . 24 2.4.2 Integrated Properties of Outflows . 26 2.4.3 Spatially Resolved Properties of Outflows . 29 2.5 Discussion . 31 2.5.1 Ionization by Star Formation vs. AGN . 31 2.5.2 Outflow Line Profiles . 32 2.5.3 Gas Velocity . 36 2.5.4 Feedback . 37 1 2.6 Summary . 40 3 Gas Kinematics 45 3.1 Introduction . 46 3.2 Data . 48 3.3 Analysis . 55 3.3.1 Spatially Resolved Spectra . 55 3.3.2 Emission Line Fluxes . 57 3.3.3 Multi-Component Velocity Measurements . 57 3.3.4 Circular Velocity Curves . 58 3.4 Results . 60 3.4.1 Comparison with NFW . 60 3.4.2 Peculiar Gas . 66 3.4.3 Star Formation Suppression . 70 3.4.4 Environment . 73 3.5 Summary . 75 4 AGN Impact on Dwarf Galaxy Stellar Populations 81 4.1 Introduction . 81 4.2 Data and Analysis . 84 4.2.1 Star Formation History . 84 4.2.2 Mass Weighted Stellar Ages and Abundances . 87 4.3 Results and Discussion . 88 4.3.1 Are AGN suppressing star formation in isolated galaxies? . 90 4.3.2 The story behind counter-rotation . 91 4.3.3 Stellar Activity and Outflows . 94 4.4 Summary . 95 5 Summary and Conclusions 100 5.1 AGN are able to expel gas from dwarf galaxies . 100 5.2 AGN can affect global gas kinematics . 101 5.3 AGN with disturbed gas are associated with star formation suppression . 102 A 105 A.1 Black Hole Masses . 105 A.2 Spatial Properties of Outflows . 106 A.3 Inclination Correction . 106 A.4 All rotation curves . 108 Bibliography 115 2 List of Figures 1.1 Figure 5 from the [47] Annual Review shows the discrepancy between pre- dicted and observed stellar mass functions. The halo mass function predicted by dark-matter-only simulations is denoted by the thick black line, and the corresponding stellar mass function assuming a constant baryonic fraction and star formation efficiency for each halo (M? = ϵ? fb Mhalo) is plotted as a dotted black line. In comparison, the observed stellar mass function of galaxies of [29] and [358] are shown as magenta stars and cyan squares, respectively. The gray shaded region depicts a range of possible faint-end slopes between α = −1:62 to −1:32. Note that the maximum star forma- 11 tion efficiency is reached in galaxies of roughly 10 M⊙, while star formation becomes increasingly inefficient at the low- and high- mass end of themass function. 3 3 2.1 Top: BPT line ratios from the central 0.2 kpc of each galaxy for dwarf galaxies in our sample observed with Keck/LRIS. 29 galaxies with optical signatures of AGN were selected from the samples of RGG13, M14, and S15.The remaining 21 are a control sample composed of star-forming dwarf galaxies. Dwarfs that present signatures of gas outflows are plotted with larger symbols. Bottom: Redshift and stellar mass distribution of our sample of dwarf galaxies. 15 2.2 SDSS color images of the 13 dwarf galaxies with spatially extended outflows. All images were generated using the SDSS DR12 finding chart tool, with the exception of NGC 1569, which is outside of the SDSS footprint. The NGC 1569 thumbnail is a PanSTARS z,g band color image rendered in the Aladin Lite Viewer with a 3’ field of view (∼ 1 kpc on a side). Each SDSS image is scaled to 10 kpc on a side and the placement of the 1 arcsecond-wide slit is shown in light gray. 16 4 2.3 Top: The spectrum of J084234.51+031930.7 is extracted from within R50 (gray). The pPXF best fit stellar continuum (red) is subtracted, leaving the residual emission spectrum (black). The flux units in this figure are (erg cm−2 s−1 Å−1). Middle: One- and two-component Gaussian fits to the [O iii] doublet are shown. The one-component model on the left is clearly a poor fit compared to the multicomponent fit on the right. The narrow (green) and broad (orange) component color scheme is used throughout this paper. Bottom: A close up of the outflow component of [O iii]λ5007 and its W80 ∼ FWHM shaded in orange, indicating the outflow velocity (dashed line) and escape velocity of this galaxy (dotted line). 20 2.4 Emission lines for J084234.51+031930.7 are shown as an example of how the kinematic components can be decomposed and placed on the BPT diagram. As described in Section 2.3.2 and illustrated in Fig. 2.3, the stellar continuum is subtracted and the residual [O iii] doublet is fit using a double Gaussian model which includes contaminating Fe i lines. The widths of Hα,Hβ, and [N ii] are fixed based on the [O iii] model, but the fluxes for each kinematic component are left as free parameters. The resulting line flux ratios for the narrow (green star) and the broad component (orange circle) are plotted on the BPT diagram (right). In this case, the model required an additional broad Hα component, which was used to obtain a black hole mass (See Appendix A.1). 23 5 2.5 Narrow and broad emission line ratios are shown for each galaxy with out- flows. The smaller symbols show the position of the bound gas (narrow component in spectrum) for each galaxy, and the larger symbols those of the outflow (broad component). In this paper, each galaxy is classified basedon its position of the outflow component in the AGN (pink circles), composite (gray diamonds), or star forming regions (cyan triangles). 25 2.6 Details of the broad component fits to the [O iii] doublets of each of the 13 galaxies with outflows are shown. The spectra are extracted from the region within the R50 of each galaxy and have all been normalized by the continuum flux just redward of [O iii]λ5007. AGN are grouped in the top figure and star forming galaxies are on the bottom. Average fit parameters, weighted by the luminosity of each narrow [O iii] line, are shown in the last panel of each section. Panels shaded in gray are classified as composite and are excluded from the AGN outflow average. Values of v0, W80, and vout are listed for each of the 13 galaxies in Table 2.1. 27 2.7 Spatial properties of the AGN-driven outflow in J090613.75+561015.5.
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